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PTF 13efv - An outburst 500 days prior to the SNHunt 275 explosion and its radiative efficiency

Ofek, E. O. and Cenko, S. B. and Shaviv, N. J. and Duggan, G. and Strotjohann, N.-L. and Rubin, A. and Kulkarni, S. R. and Gal-Yam, A. and Sullivan, M. and Cao, Y. and Nugent, P. E. and Kasliwal, M. M. and Sollerman, J. and Fransson, C. and Filippenko, A. V. and Perley, D. A. and Yaron, O. and Laher, R. (2016) PTF 13efv - An outburst 500 days prior to the SNHunt 275 explosion and its radiative efficiency. Astrophysical Journal, 824 (1). Art. No. 6. ISSN 0004-637X. https://resolver.caltech.edu/CaltechAUTHORS:20160707-105410507

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Abstract

The progenitors of some supernovae (SNe) exhibit outbursts with super-Eddington luminosities prior to their final explosions. This behavior is common among SNe IIn, but the driving mechanisms of these precursors are not yet well-understood. SNHunt 275 was announced as a possible new SN during 2015 May. Here we report on pre-explosion observations of the location of this event by the Palomar Transient Factory (PTF) and report the detection of a precursor about 500 days prior to the 2015 May activity (PTF 13efv). The observed velocities in the 2015 transient and its 2013 precursor absorption spectra are low (1000–2000 km s^(−1)), so it is not clear yet if the recent activity indeed marks the final disruption of the progenitor. Regardless of the nature of this event, we use the PTF photometric and spectral observations, as well as Swift-UVOT observations, to constrain the efficiency of the radiated energy relative to the total kinetic energy of the precursor. We find that, using an order-of-magnitude estimate and under the assumption of spherical symmetry, the ratio of the radiated energy to the kinetic energy is in the range of 4 × 10^(−2) to 3.4 × 10^3.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.3847/0004-637X/824/1/6DOIArticle
http://iopscience.iop.org/article/10.3847/0004-637X/824/1/6/metaPublisherArticle
https://arxiv.org/abs/1605.02450arXivDiscussion Paper
ORCID:
AuthorORCID
Ofek, E. O.0000-0002-6786-8774
Cenko, S. B.0000-0003-1673-970X
Duggan, G.0000-0002-9256-6735
Kulkarni, S. R.0000-0001-5390-8563
Gal-Yam, A.0000-0002-3653-5598
Sullivan, M.0000-0001-9053-4820
Cao, Y.0000-0002-8036-8491
Nugent, P. E.0000-0002-3389-0586
Kasliwal, M. M.0000-0002-5619-4938
Sollerman, J.0000-0003-1546-6615
Fransson, C.0000-0001-8532-3594
Filippenko, A. V.0000-0003-3460-0103
Perley, D. A.0000-0001-8472-1996
Yaron, O.0000-0002-0301-8017
Laher, R.0000-0003-2451-5482
Additional Information:© 2016. The American Astronomical Society. Received 2015 September 21; accepted 2016 March 7; published 2016 June 3. We thank M. Graham, P. Kelly, A. Bostroem, I. Shivvers, and W. Zheng for their help obtaining some of the optical spectra. We are also grateful to the staffs of the Palomar, Lick, and Keck Observatories for their excellent assistance. Research at Lick Observatory is partially supported by a generous gift from Google. Some of the data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA; the observatory was made possible by the generous financial support of the W.M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. E.O.O. is the incumbent of the Arye Dissentshik career development chair and is grateful for support by grants from the Willner Family Leadership Institute Ilan Gluzman (Secaucus NJ), the Israel Science Foundation, Minerva, Weizmann-UK, and the I-Core program by the Israeli Committee for Planning and Budgeting and the Israel Science Foundation (ISF). N.J.S. is grateful for the IBM Einstein Fellowship. A.G.Y. is supported by the EU/FP7 via ERC grant No. 307260, the Quantum universe I-Core program by the Israeli Committee for Planning and Budgeting and the ISF; by Minerva and ISF grants; by the Weizmann-UK "making connections" program; and by Kimmel and ARCHES awards. M.S. acknowledges support from the Royal Society and EU/FP7-ERC grant No. 615929. A.V.F.'s research is supported by the Christopher R. Redlich Fund, the TABASGO Foundation, and NSF grant AST-1211916.
Group:Infrared Processing and Analysis Center (IPAC), Palomar Transient Factory
Funders:
Funding AgencyGrant Number
GoogleUNSPECIFIED
W. M. Keck FoundationUNSPECIFIED
Willner Family Leadership Institute Ilan GluzmanUNSPECIFIED
Israel Science FoundationUNSPECIFIED
MINERVA (Israel)UNSPECIFIED
Weizmann-UKUNSPECIFIED
Israeli Committee for Planning and BudgetingUNSPECIFIED
Kimmel AwardUNSPECIFIED
Royal SocietyUNSPECIFIED
European Research Council (ERC)615929
Christopher R. Redlich FundUNSPECIFIED
TABASGO FoundationUNSPECIFIED
NSFAST-1211916
ARCHES AwardUNSPECIFIED
IBM Einstein FellowshipUNSPECIFIED
Subject Keywords:stars: mass-loss; supernovae: general; supernovae: individual (PTF13efv, SNHunt275)
Issue or Number:1
Record Number:CaltechAUTHORS:20160707-105410507
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20160707-105410507
Official Citation:E. O. Ofek et al 2016 ApJ 824 6
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:68891
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:07 Jul 2016 18:54
Last Modified:22 Nov 2019 22:25

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